KI V² Sensitivity and Observing parameters

This page contains KI sensitivity and instrument details for proposal and observation planning for V2 observations. In the V2 mode the main data product is the normalized visibility amplitude squared for a given source. Integrations on the target source and calibrators are interleaved in time, where each integration comprises fringe tracking data and all necessary calibrations. See the data overview for more details on the data.

Sensitivity information is up-to-date for 2008B proposals.

The V2 mode is open for proposals from all Keck users (UC, Caltech, UH, NASA and NOAO TACs). The sensitivity values below are based on past interferometer performance in good weather. The interferometer performance degrades substantially in poor seeing.

• Sensitivity numbers updated: March 6, 2008
• AO (adaptive optics) sensitivity:
  • R < 12 (somewhat dependent on source color, less sensitive than AO alone due to the dichroic which sends light to interferometer)
  • See the Keck Observatory AO page for more details.
  • Offset from a nearby AO star to the interferometry target is supported but this mode has a lower observing efficiency. The maximum offset is roughly 15 arcsec, but is position dependent, please contact the MSC for details. The minimum offset is ~0.2 arcsec, but see the angle tracking section for other options for closer binaries.
  • Note that the image rotators are used in vertical angle mode.

• Angle tracking:
  • 80 Hz: 5.0 < J < 10.5
  • For bright sources, an neutral density filters can be used to shift the range by up to 4.2 mags.
  • The FOV is 0.6 arcsec with a plate scale of 0.06 arcsec/pixel.
  • For binaries in which both components in are in the angle tracker FOV, a single component can be selected and sent to the fringe tracker if the separation is greater than ~0.1 arcsec. However, note that this mode results in decreased observing efficiency.

• Fringe tracking: The fringe tracker performs science observations in EITHER K (2.2 microns) or H (1.6 microns) band. Note that the frame rate must be the same for an entire cluster (target + calibrators), but that it can be changed between clusters. If an aperture is used for attenuation, it must also remain in place for the entire cluster.

  Visibility mode verification tests have shown a 0.03 systematic bias in the squared visibility. Users should not assume measurements of absolute visibility to better than this level. The spectral channel-to-channel relative visibility systematic has been measured at 0.02 in squared visibility for the 4 and 5 channels modes and 0.01 for the 10 and 42 channels modes. See the flux bias memo for more details.

  The limits below apply to unresolved targets.

  • Low resolution modes:
    • 5 pixels across K'
    • 200 Hz: 6.2 < K' < 9.9
    • 100 Hz(**): 6.6 < K' < 10.3

    • 10 pixels across K'
    • 200 Hz: 5.4 < K' < 9.1
    • 100 Hz(**): 5.8 < K' < 9.5

    • 4 pixels across H
    • 200 Hz: 5.3 < H < 9.0
  • Medium resolution mode (see additional notes)
    • 42 pixels across K'
    • 200 Hz: 3.5 < K' < 7.2
    • 100 Hz(**): 3.9 < K' < 7.6
  • (**) NOTE: The spectral channel relative visibility calibration of 0.02 has only been validated at 200 Hz. Although this is considered low risk, the 100 Hz mode may have higher relative flux errors.
  • For bright sources, an aperture can be used to shift the magnitudes by ~2.4 mags.
  • The DN-to-electron conversion is 0.26.

• Nominal fringe spacing (wavelength/baseline) for the 85 m Keck-Keck baseline:
  • K: 5.2 mas
  • H: 3.8 mas

  As KI is a fringe-tracking interferometers, all targets and calibrators must exceed a threshold visibility to be observable. The limits given above are appropriate for unresolved (i.e. point-like) sources. If the target is resolved, the instrument sensitivity decreases as shown in the table below. Targets can not be larger than 4.5 mas diameter at K band or 3.3 mas diameter at H band. Please contact the MSC if you have questions about the observability of potential targets.

  The table below gives the reduction in sensitivity (X given in magnitudes) for a given source diameter.

  X K_mag	Diameter (mas)	X H_mag	Diameter (mas)
  0.00	< 1	0.00	< 0.7
  0.25	1.6	0.25	1.2
  0.50	2.2	0.50	1.6
  0.75	2.7	0.75	2.0
  1.00	3.1	1.00	2.2
  1.25	3.4	1.25	2.5
  1.50	3.7	1.50	2.7
  1.75	3.9	1.75	2.8
  2.00	4.2	2.00	3.0

• Sky coverage:
  • Delay Range:
    • continuous (fast delay lines - FDL ): +/- 15 m
    • quasi-static (long delay lines - LDL): +/- 72m
    The total delay is calculated by summing the FDL and LDL values. Zenith pointing occurs at a delay of approx. -40 meters.

    Up to different 4 long delay line positions can be used in a single night. The long delay lines take 20 minutes to re-position and align and should be changed only between groups of targets and calibrators. The timing gui in getCal plots the detailed coverage for a given LDL position.

  • Zenith Range:
    • maximum zenith angle: 50 deg
    • 3 deg radius around zenith excluded, degraded performance is sometimes seen within 5 degrees of zenith
• Observing efficiency: For sources where all magnitudes (V,J,K) are > 1 magnitude above the sensitivity limits, KI can achieve 6 scans per hour under good weather and seeing conditions. A scan includes the fringe tracking data and calibrations. A separate scan on a nearby calibrator is required to determine the system visibility. This means that for a source/calibrator pair, there will be 3 integrations on each in an hour.

  For sources at the sensitivity limit of one of the sub-systems, the efficiency is generally closer to 4 scans per hour.

  The first 30 minutes after the domes open may be necessary for interferometer set-up and no science observations are guaranteed during this time.

• Field-of-view: ~50 mas FWHM (set by a single-mode fiber matched to the diffraction limit of a single telescope)
• Keck-Keck baseline is 85 meters and approx. 38 degrees East of North
• See the getCal planning tool to check coverage for any object.

  K-band u-v Coverage (as a function of declination):

  • Coverage given for 50 deg zenith angle range and u,v axis are in Mlambda
  • 50 deg dec
  • 35 deg dec
  • 25 deg dec
  • 15 deg dec
  • 5 deg dec
  • 0 deg dec
  • -5 deg dec
  • -15 deg dec
  • -25 deg dec